Anomalous Galactic Dynamics by Collusion of Rindler and Cosmological Horizons

Abstract

Abstract In holography, the dimensional reduction of phase space to two dimensions defines a dynamical dark energy of , associated with the cosmological horizon at a Hubble radius of , and inertia m of baryonic matter at acceleration α in terms of a thermodynamic potential of Rindler horizons at . Here, H is the Hubble parameter with deceleration q and c is the velocity of light. In weak gravity, m drops below Newton’s value m 0 as , when Rindler horizons fall beyond the cosmological horizon. The onset to weak gravity across is sharp by causality. Striking evidence is found in galaxy rotation curves, whose asymptotic dynamics is parameterized by Milgrom’s scale of acceleration . This onset presents a new challenge for canonical dark matter distributions on galactic scales in ΛCDM. Instead, future galaxy surveys may determine , to provide a direct test of dynamical dark energy ( ) versus ΛCDM ( ) and establish a bound of on the mass of the putative dark matter particle with clustering limited to galaxy clusters.